Distribution and lifetime of cosmic-ray electrons in the galaxy

When the source spectrum of cosmic-ray electrons has the form E−γ, the equilibrium spectrum is expected to approach E−γ−1 above a critical energy Ec, where Ec is a function of the storage time and the energy loss rate due to synchrotron radiation and the inverse Compton effect. The observed electron spectrum, which is a combination of the latest results of the Minnesota group, Chicago group, Bombay group, and Leiden group, can be well expressed by a single power law (~E−2.5) for 3 < E < 100 GeV. A knee observed at about 3 GeV might also be due to a solar effect.Thus the possibilities are either [Formula: see text] or Ec > 50 GeV. These two cases lead to largely different models with respect to the source spectrum, the acceleration, the storage time, and the distribution of cosmic-ray electrons in the galaxy. The radio observations are compatible with the hypothesis based on [Formula: see text].

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Interpretation of flares of red dwarfs by means of the inverse compton effect

Astrophysics ◽

10.1007/bf01004374 ◽

1980 ◽

Vol 15 (3) ◽

pp. 293-300

Author(s):

G. A. Arutyunyan ◽

R. A. Krikorian ◽

A. G. Nikogosyan

Keyword(s):

Compton Effect ◽

Inverse Compton Effect ◽

Red Dwarfs ◽

Inverse Compton

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Supernova Optical Observations and Theory

Proceedings of the International Astronomical Union ◽

10.1017/s1743921313009265 ◽

2013 ◽

Vol 9 (S296) ◽

pp. 77-85

Author(s):

Keiichi Maeda ◽

Melina C. Bersten ◽

Takashi J. Moriya ◽

Gaston Folatelli ◽

Ken'ichi Nomoto

Keyword(s):

Radioactive Decay ◽

Compton Effect ◽

Optical Observations ◽

Optical Data ◽

Frequency Data ◽

Inverse Compton Effect ◽

Inverse Compton ◽

Γ Ray ◽

Synthesized Materials

AbstractWe review emission processes within the supernova (SN) ejecta. Examples of the application of the theory to observational data are presented. The emission processes and thermal condition within the SN ejecta change as a function of time, and multi-epoch observations are important to obtain comprehensive views. Through the analyses, we can constrain the progenitor radius, compositions as a function of depth, ejecta properties, explosion asymmetry and so on. Multi-frequency follow-up is also important, including radio synchrotron emissions and the inverse Compton effect, γ-ray emissions from radioactive decay of newly synthesized materials. The optical data are essential to make the best use of the multi-frequency data.

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The Inverse Compton Effect in Extra-Galactic Radio Sources

Publications of the Astronomical Society of Australia ◽

10.1017/s1323358000010894 ◽

1968 ◽

Vol 1 (3) ◽

pp. 105-106

Author(s):

I. D. Johnston ◽

G. P. Rothman

Keyword(s):

Compton Effect ◽

Radio Sources ◽

Radiation Density ◽

X Ray ◽

Inverse Compton Scattering ◽

Ultrarelativistic Electron ◽

Inverse Compton Effect ◽

Inverse Compton ◽

Infra Red ◽

Galactic Radio

It was first pointed out by Hoyle et al. that quasars if they are indeed located at cosmological distances, must be characterized by an extraordinarily large radiation density : and therefore, though their optical and near infra-red spectra appear to be dominated by synchrotron radiation, any ultrarelativistic electron present must necessarily lose essentially all its energy by inverse Compton scattering. This would mean that, though quasars are emitting fantastic amounts of energy at optical frequencies, they must also be emitting many orders of magnitude more at X-ray and γ-ray frequencies. This paradox has been evaded by several specially constructed models (e.g. Rees and Sciama, Woltjer and Jukes); but the problem has not been removed in general.

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